Abstract
Abstract Kaba meteorite as a reference material (one of a least metamorphosed and most primitive carbonaceous chondrites fell on Earth) was chosen for this study providing an adequate background for study of the protoplanetary disk or even the crystallization processes of the Early Solar System. Its olivine minerals (forsterite and fayalite) and their Mg/Fe ratio can help us to understand more about the planet formation mechanism and whether or not the metallic constitutes of the disk could be precursors for the type of planets in the Solar System. A multiple methodological approach such as a combination of the scanning electron microscope, optical microscope, Raman spectroscopy and electron microprobe of the olivine grains give the Fe/Mg ratio database. The analyses above confirmed that planet formation in the protoplanetary disk is driven by the mineralogical precursors of the crystallization process. On the other hand, four nebulae mentioned in this study provide the astronomical data confirming that the planet formation in the protoplanetary disk is dominated or even driven by the metallic constituents.
Highlights
Mg, Si and Fe are the most important mineral-forming elements in the Solar System, which play a dominant role in the buildup of the mantle, as well as, the crust of silicaterich planets
Kaba meteorite as a reference material was chosen for this study providing an adequate background for study of the protoplanetary disk or even the crystallization processes of the Early Solar System
Four nebulae mentioned in this study provide the astronomical data confirming that the planet formation in the protoplanetary disk is dominated or even driven by the metallic constituents
Summary
Si and Fe are the most important mineral-forming elements in the Solar System, which play a dominant role in the buildup of the mantle, as well as, the crust of silicaterich planets. Astronomical observations support that the interstellar silicates are Mg-rich (Min et al 2007), due to the higher abundance of Mg as opposed to that of Fe. Note that, the Mg/Fe ratio for the case of a highly forsteritic olivine (Fo=0.99) with a small amount of Fe can be described by the formulation of Mg(2−2x) Fe2xSiO4 where x=0.01. The major components of a typical carbonaceous chondrite (CC) are the chondrules, the interstitial fine-grained matrix consisting of hydrous and anhydrous silicates, oxides, sulfides, metals and organic matter, the Ca-Al-rich inclusions (CAIs), the amoeboid olivine aggregates (AOA), and isolated grains with forsteritic- and fayalitic olivine composition embedded in the matrix, respectively. CCs may contain a small amount of silicon carbide, which is a very characteristic carbon-based compound in meteorites containing presolar grains from the AGB stars, supernovae, and novae (Gilmour 2003)
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